We present a dust spectral energy distribution ( SED ) and binary stellar population analysis revisiting the dust production rates ( DPRs ) in the winds of carbon-rich Wolf-Rayet ( WC ) binaries and their impact on galactic dust budgets . DustEM SED models of 19 Galactic WC “ dustars ” reveal DPRs of \dot { M } _ { d } \sim 10 ^ { -10 } -10 ^ { -6 } M _ { \odot } yr ^ { -1 } and carbon dust condensation fractions , \chi _ { C } , between 0.002 - 40 \% . A large ( 0.1 - 1.0 \mu m ) dust grain size composition is favored for efficient dustars where \chi _ { C } \gtrsim 1 \% . Results for dustars with known orbital periods verify a power-law relation between \chi _ { C } , orbital period , WC mass-loss rate , and wind velocity consistent with predictions from theoretical models of dust formation in colliding-wind binaries . We incorporated dust production into Binary Population and Spectral Synthesis ( BPASS ) models to analyze dust production rates from WC dustars , asymptotic giant branch stars ( AGBs ) , red supergiants ( RSGs ) , and core-collapse supernovae ( SNe ) . BPASS models assuming constant star formation ( SF ) and a co-eval 10 ^ { 6 } M _ { \odot } stellar population were performed at low , Large Magellanic Cloud ( LMC ) -like , and solar metallicities ( Z = 0.001 , 0.008 , and 0.020 ) . Both constant SF and co-eval models show that SNe are net dust destroyers at all metallicities . Constant SF models at LMC-like metallicities show that AGB stars slightly outproduce WC binaries and RSGs by factors of 2 - 3 , whereas at solar metallicites WC binaries are the dominant source of dust for \sim 60 Myr until the onset of AGBs , which match the dust input of WC binaries . Co-eval population models show that for “ bursty ” SF , AGB stars dominate dust production at late times ( t \gtrsim 70 Myr ) .